Are Faint Supernovae Responsible for Carbon-enhanced Metal-poor Stars?

Komiya, Yutaka; Suda, Takuma; Yamada, Shimako; Fujimoto, Masayuki Y.

doi:10.3847/1538-4357/ab67be

Cited by 22 publications

(22 citation statements)

References 66 publications

(78 reference statements)

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“…Most systems from our models are below the critical absolute carbon abundance 20 A(C) = 7.1 introduced by Yoon et al (2016) to distinguish CEMP-no and CEMP-s/rs stars, consistent with the picture that CEMPno stars trace primordial enrichment while CEMP-s/rs stars are mostly explained by external enrichment in binaries (e.g. Komiya et al 2020). The difference between rotating and non-rotating models are insignificant when all stars explode as SNe, while if only stars with m > 25 M become SNe, the rotation model produces less carbon compared with the rotation model.…”

Section: Fiducial Model Of Imf and Sfesupporting

confidence: 85%

“…3.1) and AC haloes (Sec. 3.2), in comparison with previous theoretical models and observations (Cooke & Madau 2014;Yoon et al 2016;Komiya et al 2020;Jeon et al 2021). We focus particularly on the effects of winds, and reproducing the observed population of CEMP-no stars as the bona-fide footprints of primordial metal enrichment.…”

Section: Chemical Signatures Of Primordial Metal Enrichmentmentioning

confidence: 70%

“…We further investigate the scenario of faint SNe. Similar to the idealized treatment in Komiya et al (2020), to capture the fallback-mixing effect, we multiply the iron yield by a factor fFe,ej, randomly generated from a power-law distribution with index α fSN = −1/2 in the range [10 −5 , 1] for each SN, leaving the yields of other elements unchanged. The distribution of fFe,ej is chosen to reproduce the shape of the observed distribution of [Fe/H] for CEMP-no stars at [Fe/H] −4 in the fiducial cluster model for self-enriched minihaloes (see below).…”

Section: Pop III Cluster Modelmentioning

confidence: 99%

“…The first two scenarios have been extensively studied in the context of cosmic structure formation with semianalytical models and cosmological simulations (e.g. Cooke & Madau 2014;Sarmento et al 2016;Sharma et al 2018;Komiya et al 2020;Chiaki et al 2020;Jeon et al 2021), which can indeed reproduce the observed distribution of CEMP-no stars in the carbon enhancement and iron abundance space (with certain parameter choices). On the contrary, the metal enrichment process driven by Pop III stellar winds has not been investigated in any detail yet.…”

Section: Introductionmentioning

confidence: 99%

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Stellar winds and metal enrichment from fast-rotating Population III stars

Liu,

Sibony,

Meynet

et al. 2021

Preprint

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Stellar winds from fast-rotating Population III (Pop III) stars have long been suspected to make important contributions to early metal enrichment, as features in the nucleosynthesis of such 'spinstars' are consistent with the chemical abundance patterns of some metal-poor stars in the local Universe. Particularly, stellar winds rich in light elements can provide another pathway towards explaining the carbon enhancement in carbon-enhanced metal-poor (CEMP) stars. In this work, we focus on the feedback of Pop III stellar winds combined with supernovae (SNe), and derive the resulting chemical signatures in the enriched medium. We explore a large parameter space of Pop III star formation and feedback with a semi-analytical model. The predicted pattern of carbon and iron abundances of second-generation stars agrees well with observations of CEMP-no stars ([Ba/Fe] < 0) at [Fe/H] −3 and A(C) 7, under the optimistic assumption of significant mass loss by winds. In this scenario, carbon-rich but ironfree second-generation stars can form in systems dominated by enrichment from winds, gaining trace amounts of iron by accretion from the interstellar medium, to become the most iron-poor and carbon-enhanced stars seen in observations ([Fe/H] −4, [C/Fe] 2). Wind feedback from Pop III spinstars deserves more detailed modelling in early cosmic structure formation.

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Section: Fiducial Model Of Imf and Sfesupporting

confidence: 85%

Section: Chemical Signatures Of Primordial Metal Enrichmentmentioning

confidence: 70%

Section: Pop III Cluster Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Stellar winds and metal enrichment from fast-rotating Population III stars

Liu,

Sibony,

Meynet

et al. 2021

Preprint

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“…During the preparation of this manuscript, Komiya et al (2020) derived a similar estimate for the minimal dilution and implemented it into a semi-analytical model of the formation of the Milky Way. While we apply this estimate to the exploration of progenitor scenarios of individual stars, Komiya et al (2020) focus on the chemical evolution of the Milky Way and in particular on whether the overall population of CEMP-no stars can be reproduced. They find it difficult to reproduce the prevalence of large carbon abundances in the lowest metallicity stars with faint SNe.…”

Section: Discussion and Summarymentioning

confidence: 99%

A minimum dilution scenario for supernovae and consequences for extremely metal-poor stars

Magg

Nordlander

Glover

et al. 2020

Monthly Notices of the Royal Astronomical Society

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To date no metal-free stars have been identified by direct observations. The most common method of constraining their properties is searching the spectra of the most metal-poor stars for the chemical elements created in the first stars and their supernova. In this approach, modelled supernova yields are compared to the observed abundance patterns in extremely metal-poor stars. The method typically only uses the abundance ratios, i.e., the yields are diluted to the observed level. Following the usual assumption of spherical symmetry we compute a simple lower limit of the mass a supernova can mix with and find that it is consistent with all published simulations of early chemical enrichment in the interstellar medium. For three different cases, we demonstrate that this dilution limit can change the conclusions from the abundance fitting. There is a large discrepancy between the dilution found in simulations of SN explosions in minihaloes and the dilution assumed in many abundance fits. Limiting the dilution can significantly alter the likelihood of which supernovae are possible progenitors of observed CEMP-no stars. In particular, some of the faint, very low-yield SNe, which have been suggested as models for the abundance pattern of SMSS0313-6708, cannot explain the measured metal abundances, as their predicted metal yields are too small by two orders of magnitude. Altogether, the new dilution model presented here emphasizes the need to better understand the mixing and dilution behaviour of aspherical SNe.

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The evolution of CNO elements in galaxies

Romano

2022

Astron Astrophys Rev

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After hydrogen and helium, oxygen, carbon, and nitrogen—hereinafter, the CNO elements—are the most abundant species in the universe. They are observed in all kinds of astrophysical environments, from the smallest to the largest scales, and are at the basis of all known forms of life, hence, the constituents of any biomarker. As such, their study proves crucial in several areas of contemporary astrophysics, extending to astrobiology. In this review, I will summarize current knowledge about CNO element evolution in galaxies, starting from our home, the Milky Way. After a brief recap of CNO synthesis in stars, I will present the comparison between chemical evolution model predictions and observations of CNO isotopic abundances and abundance ratios in stars and in the gaseous matter. Such a comparison permits to constrain the modes and time scales of the assembly of galaxies and their stellar populations, as well as stellar evolution and nucleosynthesis theories. I will stress that chemical evolution models must be carefully calibrated against the wealth of abundance data available for the Milky Way before they can be applied to the interpretation of observational datasets for other systems. In this vein, I will also discuss the usefulness of some key CNO isotopic ratios as probes of the prevailing, galaxy-wide stellar initial mass function in galaxies where more direct estimates from the starlight are unfeasible.

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Are Faint Supernovae Responsible for Carbon-enhanced Metal-poor Stars?

Cited by 22 publications

References 66 publications

Stellar winds and metal enrichment from fast-rotating Population III stars

Stellar winds and metal enrichment from fast-rotating Population III stars

A minimum dilution scenario for supernovae and consequences for extremely metal-poor stars

The evolution of CNO elements in galaxies

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